Chromium isotopic insights into the origin of chondrite parent bodies and the early terrestrial volatile depletion

Ke Zhu; Frédéric Moynier; Martin Schiller; Conel M.O.D. Alexander; Jemma Davidson; Devin L. Schrader; Elishevah van Kooten; Martin Bizzarro

doi:10.1016/j.gca.2021.02.031

Chromium isotopic insights into the origin of chondrite parent bodies and the early terrestrial volatile depletion

Ke Zhu^*, Frédéric Moynier, Martin Schiller, Conel M.O.D. Alexander, Jemma Davidson, Devin L. Schrader, Elishevah van Kooten, Martin Bizzarro

^*Corresponding author for this work

School of Earth Sciences

Research output: Contribution to journal › Article (Academic Journal) › peer-review

50 Citations (Scopus)

Abstract

Chondrites are meteorites from undifferentiated parent bodies that provide fundamental information about early Solar System evolution and planet formation. The element Cr is highly suitable for deciphering both the timing of formation and the origin of planetary building blocks because it records both radiogenic contributions from ⁵³Mn-⁵³Cr decay and variable nucleosynthetic contributions from the stable ⁵⁴Cr nuclide. Here, we report high-precision measurements of the mass-independent Cr isotope compositions (ε⁵³Cr and ε⁵⁴Cr) of chondrites (including all carbonaceous chondrites groups) and terrestrial samples using for the first time a multi-collection inductively-coupled-plasma mass-spectrometer to better understand the formation histories and genetic relationships between chondrite parent bodies. With our comprehensive dataset, the order of decreasing ε⁵⁴Cr (per ten thousand deviation of the ⁵⁴Cr/⁵²Cr ratio relative to a terrestrial standard) values amongst the carbonaceous chondrites is updated to CI = CH ≥ CB ≥ CR ≥ CM ≈ CV ≈ CO ≥ CK > EC > OC. Chondrites from CO, CV, CR, CM and CB groups show intra-group ε⁵⁴Cr heterogeneities that may result from sample heterogeneity and/or heterogeneous accretion of their parent bodies. Resolvable ε⁵⁴Cr (with 2SE uncertainty) differences between CV and CK chondrites rule out an origin from a common parent body or reservoir as has previously been suggested. The CM and CO chondrites share common ε⁵⁴Cr characteristics, which suggests their parent bodies may have accreted their components in similar proportions. The CB and CH chondrites have low-Mn/Cr ratios and similar ε⁵³Cr values to the CI chondrites, invalidating them as anchors for a bulk ⁵³Mn-⁵³Cr isochron for carbonaceous chondrites. Bulk Earth has a ε⁵³Cr value that is lower than the average of chondrites, including enstatite chondrites. This depletion may constrain the timing of volatile loss from the Earth or its precursors to be within the first million years of Solar System formation and is incompatible with Earth's accretion via any of the known chondrite groups as main contributors, including enstatite chondrites.

Original language	English
Pages (from-to)	158-186
Number of pages	29
Journal	Geochimica et Cosmochimica Acta
Volume	301
Early online date	15 Apr 2021
DOIs	https://doi.org/10.1016/j.gca.2021.02.031
Publication status	Published - 15 May 2021

Bibliographical note

Funding Information:
We deeply appreciate Thorsten Kleine for efficient editorial handling and detailed and constructive comments from Herbert Palme, Anne Trinquier and one anonymous reviewer, which greatly improved this manuscript. F. M. acknowledges funding from the European Research Council under the H2020 framework program/ERC grant agreement (#637503-PRISTINE) and financial support of the UnivEarthS Labex program at Sorbonne Paris Cité (#ANR-10-LABX-0023 and #ANR-11-IDEX-0005-02), and the ANR through a chaire d'excellence Sorbonne Paris Cité. Parts of this work were supported by IPGP multidisciplinary program PARI, and by Paris–IdF region SESAME (#12015908). M. B. acknowledges funding from the Carlsberg Foundation (CF18-1105), the Danish National Research Foundation (DNRF97) and the European Research Council (ERC Advanced Grant Agreement, #833275-DEEPTIME). M. S. acknowledges funding from the Villum Fonden (#00025333). E.v.K. acknowledges funding from the European Union's Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie Grant Agreement No 786081. We also appreciate the Arizona State University Center for Meteorite Studies for providing some of the samples used in this study. US Antarctic meteorite samples are recovered by the Antarctic Search for Meteorites (ANSMET) program which has been funded by NSF and NASA, and characterized and curated by the Department of Mineral Sciences of the Smithsonian Institution and Astromaterials Acquisition and Curation Office at NASA Johnson Space Center. Timothy Mock is appreciated for providing the Cr isotope standard of NIST SRM 3112a. K. Z. thanks the China Scholarship Council (CSC) and IPGP for a PhD fellowship (#201706340161) and the Aide à la MOBILITE INTERNATIONALE des doctorants de l'IPGP (2019), respectively.

Funding Information:
We deeply appreciate Thorsten Kleine for efficient editorial handling and detailed and constructive comments from Herbert Palme, Anne Trinquier and one anonymous reviewer, which greatly improved this manuscript. F. M. acknowledges funding from the European Research Council under the H2020 framework program/ERC grant agreement (#637503-PRISTINE) and financial support of the UnivEarthS Labex program at Sorbonne Paris Cité (#ANR-10-LABX-0023 and #ANR-11-IDEX-0005-02), and the ANR through a chaire d’excellence Sorbonne Paris Cité. Parts of this work were supported by IPGP multidisciplinary program PARI, and by Paris–IdF region SESAME (#12015908). M. B. acknowledges funding from the Carlsberg Foundation (CF18-1105), the Danish National Research Foundation (DNRF97) and the European Research Council (ERC Advanced Grant Agreement, #833275-DEEPTIME). M. S. acknowledges funding from the Villum Fonden (#00025333). E.v.K. acknowledges funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie Grant Agreement No 786081. We also appreciate the Arizona State University Center for Meteorite Studies for providing some of the samples used in this study. US Antarctic meteorite samples are recovered by the Antarctic Search for Meteorites (ANSMET) program which has been funded by NSF and NASA, and characterized and curated by the Department of Mineral Sciences of the Smithsonian Institution and Astromaterials Acquisition and Curation Office at NASA Johnson Space Center. Timothy Mock is appreciated for providing the Cr isotope standard of NIST SRM 3112a. K. Z. thanks the China Scholarship Council (CSC) and IPGP for a PhD fellowship (#201706340161) and the Aide à la MOBILITE INTERNATIONALE des doctorants de l’IPGP (2019), respectively.

Publisher Copyright:
© 2021 Elsevier Ltd

Keywords

Mn-Cr chronometry
Cr systematics
Chondrites
Condensation history
CV subgroups
CV-CK, CH-CB and CO-CM clans
Early Earth
Genetic relationship
Solar System
Volatile depletion

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@article{ea10f3eea07f4b33bba024a366ab025b,

title = "Chromium isotopic insights into the origin of chondrite parent bodies and the early terrestrial volatile depletion",

abstract = "Chondrites are meteorites from undifferentiated parent bodies that provide fundamental information about early Solar System evolution and planet formation. The element Cr is highly suitable for deciphering both the timing of formation and the origin of planetary building blocks because it records both radiogenic contributions from 53Mn-53Cr decay and variable nucleosynthetic contributions from the stable 54Cr nuclide. Here, we report high-precision measurements of the mass-independent Cr isotope compositions (ε53Cr and ε54Cr) of chondrites (including all carbonaceous chondrites groups) and terrestrial samples using for the first time a multi-collection inductively-coupled-plasma mass-spectrometer to better understand the formation histories and genetic relationships between chondrite parent bodies. With our comprehensive dataset, the order of decreasing ε54Cr (per ten thousand deviation of the 54Cr/52Cr ratio relative to a terrestrial standard) values amongst the carbonaceous chondrites is updated to CI = CH ≥ CB ≥ CR ≥ CM ≈ CV ≈ CO ≥ CK > EC > OC. Chondrites from CO, CV, CR, CM and CB groups show intra-group ε54Cr heterogeneities that may result from sample heterogeneity and/or heterogeneous accretion of their parent bodies. Resolvable ε54Cr (with 2SE uncertainty) differences between CV and CK chondrites rule out an origin from a common parent body or reservoir as has previously been suggested. The CM and CO chondrites share common ε54Cr characteristics, which suggests their parent bodies may have accreted their components in similar proportions. The CB and CH chondrites have low-Mn/Cr ratios and similar ε53Cr values to the CI chondrites, invalidating them as anchors for a bulk 53Mn-53Cr isochron for carbonaceous chondrites. Bulk Earth has a ε53Cr value that is lower than the average of chondrites, including enstatite chondrites. This depletion may constrain the timing of volatile loss from the Earth or its precursors to be within the first million years of Solar System formation and is incompatible with Earth's accretion via any of the known chondrite groups as main contributors, including enstatite chondrites.",

keywords = "Mn-Cr chronometry, Cr systematics, Chondrites, Condensation history, CV subgroups, CV-CK, CH-CB and CO-CM clans, Early Earth, Genetic relationship, Solar System, Volatile depletion",

author = "Ke Zhu and Fr{\'e}d{\'e}ric Moynier and Martin Schiller and Alexander, {Conel M.O.D.} and Jemma Davidson and Schrader, {Devin L.} and {van Kooten}, Elishevah and Martin Bizzarro",

note = "Funding Information: We deeply appreciate Thorsten Kleine for efficient editorial handling and detailed and constructive comments from Herbert Palme, Anne Trinquier and one anonymous reviewer, which greatly improved this manuscript. F. M. acknowledges funding from the European Research Council under the H2020 framework program/ERC grant agreement (#637503-PRISTINE) and financial support of the UnivEarthS Labex program at Sorbonne Paris Cit{\'e} (#ANR-10-LABX-0023 and #ANR-11-IDEX-0005-02), and the ANR through a chaire d'excellence Sorbonne Paris Cit{\'e}. Parts of this work were supported by IPGP multidisciplinary program PARI, and by Paris–IdF region SESAME (#12015908). M. B. acknowledges funding from the Carlsberg Foundation (CF18-1105), the Danish National Research Foundation (DNRF97) and the European Research Council (ERC Advanced Grant Agreement, #833275-DEEPTIME). M. S. acknowledges funding from the Villum Fonden (#00025333). E.v.K. acknowledges funding from the European Union's Horizon 2020 research and innovation programme under the Marie Sk{\l}odowska-Curie Grant Agreement No 786081. We also appreciate the Arizona State University Center for Meteorite Studies for providing some of the samples used in this study. US Antarctic meteorite samples are recovered by the Antarctic Search for Meteorites (ANSMET) program which has been funded by NSF and NASA, and characterized and curated by the Department of Mineral Sciences of the Smithsonian Institution and Astromaterials Acquisition and Curation Office at NASA Johnson Space Center. Timothy Mock is appreciated for providing the Cr isotope standard of NIST SRM 3112a. K. Z. thanks the China Scholarship Council (CSC) and IPGP for a PhD fellowship (#201706340161) and the Aide {\`a} la MOBILITE INTERNATIONALE des doctorants de l'IPGP (2019), respectively. Funding Information: We deeply appreciate Thorsten Kleine for efficient editorial handling and detailed and constructive comments from Herbert Palme, Anne Trinquier and one anonymous reviewer, which greatly improved this manuscript. F. M. acknowledges funding from the European Research Council under the H2020 framework program/ERC grant agreement (#637503-PRISTINE) and financial support of the UnivEarthS Labex program at Sorbonne Paris Cit{\'e} (#ANR-10-LABX-0023 and #ANR-11-IDEX-0005-02), and the ANR through a chaire d{\textquoteright}excellence Sorbonne Paris Cit{\'e}. Parts of this work were supported by IPGP multidisciplinary program PARI, and by Paris–IdF region SESAME (#12015908). M. B. acknowledges funding from the Carlsberg Foundation (CF18-1105), the Danish National Research Foundation (DNRF97) and the European Research Council (ERC Advanced Grant Agreement, #833275-DEEPTIME). M. S. acknowledges funding from the Villum Fonden (#00025333). E.v.K. acknowledges funding from the European Union{\textquoteright}s Horizon 2020 research and innovation programme under the Marie Sk{\l}odowska-Curie Grant Agreement No 786081. We also appreciate the Arizona State University Center for Meteorite Studies for providing some of the samples used in this study. US Antarctic meteorite samples are recovered by the Antarctic Search for Meteorites (ANSMET) program which has been funded by NSF and NASA, and characterized and curated by the Department of Mineral Sciences of the Smithsonian Institution and Astromaterials Acquisition and Curation Office at NASA Johnson Space Center. Timothy Mock is appreciated for providing the Cr isotope standard of NIST SRM 3112a. K. Z. thanks the China Scholarship Council (CSC) and IPGP for a PhD fellowship (#201706340161) and the Aide {\`a} la MOBILITE INTERNATIONALE des doctorants de l{\textquoteright}IPGP (2019), respectively. Publisher Copyright: {\textcopyright} 2021 Elsevier Ltd",

year = "2021",

month = may,

day = "15",

doi = "10.1016/j.gca.2021.02.031",

language = "English",

volume = "301",

pages = "158--186",

journal = "Geochimica et Cosmochimica Acta",

issn = "0016-7037",

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TY - JOUR

T1 - Chromium isotopic insights into the origin of chondrite parent bodies and the early terrestrial volatile depletion

AU - Zhu, Ke

AU - Moynier, Frédéric

AU - Schiller, Martin

AU - Alexander, Conel M.O.D.

AU - Davidson, Jemma

AU - Schrader, Devin L.

AU - van Kooten, Elishevah

AU - Bizzarro, Martin

N1 - Funding Information: We deeply appreciate Thorsten Kleine for efficient editorial handling and detailed and constructive comments from Herbert Palme, Anne Trinquier and one anonymous reviewer, which greatly improved this manuscript. F. M. acknowledges funding from the European Research Council under the H2020 framework program/ERC grant agreement (#637503-PRISTINE) and financial support of the UnivEarthS Labex program at Sorbonne Paris Cité (#ANR-10-LABX-0023 and #ANR-11-IDEX-0005-02), and the ANR through a chaire d'excellence Sorbonne Paris Cité. Parts of this work were supported by IPGP multidisciplinary program PARI, and by Paris–IdF region SESAME (#12015908). M. B. acknowledges funding from the Carlsberg Foundation (CF18-1105), the Danish National Research Foundation (DNRF97) and the European Research Council (ERC Advanced Grant Agreement, #833275-DEEPTIME). M. S. acknowledges funding from the Villum Fonden (#00025333). E.v.K. acknowledges funding from the European Union's Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie Grant Agreement No 786081. We also appreciate the Arizona State University Center for Meteorite Studies for providing some of the samples used in this study. US Antarctic meteorite samples are recovered by the Antarctic Search for Meteorites (ANSMET) program which has been funded by NSF and NASA, and characterized and curated by the Department of Mineral Sciences of the Smithsonian Institution and Astromaterials Acquisition and Curation Office at NASA Johnson Space Center. Timothy Mock is appreciated for providing the Cr isotope standard of NIST SRM 3112a. K. Z. thanks the China Scholarship Council (CSC) and IPGP for a PhD fellowship (#201706340161) and the Aide à la MOBILITE INTERNATIONALE des doctorants de l'IPGP (2019), respectively. Funding Information: We deeply appreciate Thorsten Kleine for efficient editorial handling and detailed and constructive comments from Herbert Palme, Anne Trinquier and one anonymous reviewer, which greatly improved this manuscript. F. M. acknowledges funding from the European Research Council under the H2020 framework program/ERC grant agreement (#637503-PRISTINE) and financial support of the UnivEarthS Labex program at Sorbonne Paris Cité (#ANR-10-LABX-0023 and #ANR-11-IDEX-0005-02), and the ANR through a chaire d’excellence Sorbonne Paris Cité. Parts of this work were supported by IPGP multidisciplinary program PARI, and by Paris–IdF region SESAME (#12015908). M. B. acknowledges funding from the Carlsberg Foundation (CF18-1105), the Danish National Research Foundation (DNRF97) and the European Research Council (ERC Advanced Grant Agreement, #833275-DEEPTIME). M. S. acknowledges funding from the Villum Fonden (#00025333). E.v.K. acknowledges funding from the European Union’s Horizon 2020 research and innovation programme under the Marie Skłodowska-Curie Grant Agreement No 786081. We also appreciate the Arizona State University Center for Meteorite Studies for providing some of the samples used in this study. US Antarctic meteorite samples are recovered by the Antarctic Search for Meteorites (ANSMET) program which has been funded by NSF and NASA, and characterized and curated by the Department of Mineral Sciences of the Smithsonian Institution and Astromaterials Acquisition and Curation Office at NASA Johnson Space Center. Timothy Mock is appreciated for providing the Cr isotope standard of NIST SRM 3112a. K. Z. thanks the China Scholarship Council (CSC) and IPGP for a PhD fellowship (#201706340161) and the Aide à la MOBILITE INTERNATIONALE des doctorants de l’IPGP (2019), respectively. Publisher Copyright: © 2021 Elsevier Ltd

PY - 2021/5/15

Y1 - 2021/5/15

N2 - Chondrites are meteorites from undifferentiated parent bodies that provide fundamental information about early Solar System evolution and planet formation. The element Cr is highly suitable for deciphering both the timing of formation and the origin of planetary building blocks because it records both radiogenic contributions from 53Mn-53Cr decay and variable nucleosynthetic contributions from the stable 54Cr nuclide. Here, we report high-precision measurements of the mass-independent Cr isotope compositions (ε53Cr and ε54Cr) of chondrites (including all carbonaceous chondrites groups) and terrestrial samples using for the first time a multi-collection inductively-coupled-plasma mass-spectrometer to better understand the formation histories and genetic relationships between chondrite parent bodies. With our comprehensive dataset, the order of decreasing ε54Cr (per ten thousand deviation of the 54Cr/52Cr ratio relative to a terrestrial standard) values amongst the carbonaceous chondrites is updated to CI = CH ≥ CB ≥ CR ≥ CM ≈ CV ≈ CO ≥ CK > EC > OC. Chondrites from CO, CV, CR, CM and CB groups show intra-group ε54Cr heterogeneities that may result from sample heterogeneity and/or heterogeneous accretion of their parent bodies. Resolvable ε54Cr (with 2SE uncertainty) differences between CV and CK chondrites rule out an origin from a common parent body or reservoir as has previously been suggested. The CM and CO chondrites share common ε54Cr characteristics, which suggests their parent bodies may have accreted their components in similar proportions. The CB and CH chondrites have low-Mn/Cr ratios and similar ε53Cr values to the CI chondrites, invalidating them as anchors for a bulk 53Mn-53Cr isochron for carbonaceous chondrites. Bulk Earth has a ε53Cr value that is lower than the average of chondrites, including enstatite chondrites. This depletion may constrain the timing of volatile loss from the Earth or its precursors to be within the first million years of Solar System formation and is incompatible with Earth's accretion via any of the known chondrite groups as main contributors, including enstatite chondrites.

AB - Chondrites are meteorites from undifferentiated parent bodies that provide fundamental information about early Solar System evolution and planet formation. The element Cr is highly suitable for deciphering both the timing of formation and the origin of planetary building blocks because it records both radiogenic contributions from 53Mn-53Cr decay and variable nucleosynthetic contributions from the stable 54Cr nuclide. Here, we report high-precision measurements of the mass-independent Cr isotope compositions (ε53Cr and ε54Cr) of chondrites (including all carbonaceous chondrites groups) and terrestrial samples using for the first time a multi-collection inductively-coupled-plasma mass-spectrometer to better understand the formation histories and genetic relationships between chondrite parent bodies. With our comprehensive dataset, the order of decreasing ε54Cr (per ten thousand deviation of the 54Cr/52Cr ratio relative to a terrestrial standard) values amongst the carbonaceous chondrites is updated to CI = CH ≥ CB ≥ CR ≥ CM ≈ CV ≈ CO ≥ CK > EC > OC. Chondrites from CO, CV, CR, CM and CB groups show intra-group ε54Cr heterogeneities that may result from sample heterogeneity and/or heterogeneous accretion of their parent bodies. Resolvable ε54Cr (with 2SE uncertainty) differences between CV and CK chondrites rule out an origin from a common parent body or reservoir as has previously been suggested. The CM and CO chondrites share common ε54Cr characteristics, which suggests their parent bodies may have accreted their components in similar proportions. The CB and CH chondrites have low-Mn/Cr ratios and similar ε53Cr values to the CI chondrites, invalidating them as anchors for a bulk 53Mn-53Cr isochron for carbonaceous chondrites. Bulk Earth has a ε53Cr value that is lower than the average of chondrites, including enstatite chondrites. This depletion may constrain the timing of volatile loss from the Earth or its precursors to be within the first million years of Solar System formation and is incompatible with Earth's accretion via any of the known chondrite groups as main contributors, including enstatite chondrites.

KW - Mn-Cr chronometry

KW - Cr systematics

KW - Chondrites

KW - Condensation history

KW - CV subgroups

KW - CV-CK, CH-CB and CO-CM clans

KW - Early Earth

KW - Genetic relationship

KW - Solar System

KW - Volatile depletion

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U2 - 10.1016/j.gca.2021.02.031

DO - 10.1016/j.gca.2021.02.031

M3 - Article (Academic Journal)

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SN - 0016-7037

VL - 301

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JO - Geochimica et Cosmochimica Acta

JF - Geochimica et Cosmochimica Acta

ER -

Chromium isotopic insights into the origin of chondrite parent bodies and the early terrestrial volatile depletion

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